For the latter Wino model, the Galactic center would be the most
promising object to detect gamma rays from the DM
annihilation [1]}, [2]}.See
also [3]} for constraints on the lightest
superparticle in the pMSSM analysis using signals from the Galactic
center. In addition, see Ref. [4]} that compares
the sensitivity of observing the Galactic center and the selected
dSphs, Draco and Triangulum II. On the other hand, dSphs are also
considered to be one of the most important targets for the DM search
with the Cherenkov Telescope Array (CTA)
observatory [5]}, [6]}. Yet, as far as we are
aware, no dedicated study on the CTA sensitivity estimates for the
Wino DM searches has been performed. We, therefore, show sensitivity
projection for the CTA North for several classical and ultrafaint
dSphs. Even though the velocity dependence can be safely ignored for
the Wino masses much heavier than the gauge boson mass, the resultant
J factor changes, for example, by a factor of 1.8 between adopting
priors with \(V_{50}=18\)  km s\(^{-1}\)  and \(10.5\)  km s\(^{-1}\)  for
Reticulum II. Eventually it is found that both classical and
ultrafaint dSphs are promising targets to detect the Wino DM with
2.7–3 TeV masses, providing a complementary method to the observation
of the Galactic center.
